Neutron-Rich Nuclei in Heaven and Earth

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dc.creatorTodd-Rutel, B. G.
dc.creatorPiekarewicz, J.
dc.date2005-04-11
dc.date.accessioned2026-07-07T06:19:12Z
dc.date.available2026-07-07T06:19:12Z
dc.descriptionAn accurately calibrated relativistic parametrization is introduced to compute the ground state properties of finite nuclei, their linear response, and the structure of neutron stars. While similar in spirit to the successful NL3 parameter set, it produces an equation of state that is considerably softer -- both for symmetric nuclear matter and for the symmetry energy. This softening appears to be required for an accurate description of several collective modes having different neutron-to-proton ratios. Among the predictions of this model are a symmetric nuclear-matter incompressibility of K=230 MeV and a neutron skin thickness in 208Pb of Rn-Rp=0.21 fm. Further, the impact of such a softening on the properties of neutron stars is as follows: the model predicts a limiting neutron star mass of Mmax=1.72 Msun, a radius of R=12.66 km for a ``canonical'' M=1.4 Msun neutron star, and no (nucleon) direct Urca cooling in neutrons stars with masses below M=1.3 Msun.
dc.description4 pages, 3 tables, and no figures
dc.identifierhttps://arxiv.org/abs/nucl-th/0504034
dc.identifierhttp://arxiv.org/abs/nucl-th/0504034
dc.identifierPhys. Rev. Lett. 95, 122501 (2005)
dc.identifierdoi:10.1103/PhysRevLett.95.122501
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/94995
dc.subjectNuclear Theory
dc.subjectAstrophysics
dc.subjectNuclear Experiment
dc.titleNeutron-Rich Nuclei in Heaven and Earth
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